Whistler scattering of suprathermal electrons in the solar wind: Particle-in-cell simulations

Physics – Plasma Physics

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Space Plasma Physics: Wave/Particle Interactions (2483, 6984), Space Plasma Physics: Kinetic Waves And Instabilities, Space Plasma Physics: Nonlinear Phenomena (4400, 6944), Interplanetary Physics: Plasma Waves And Turbulence, Interplanetary Physics: Solar Wind Plasma

Scientific paper

Solar wind observations sometimes show that suprathermal, magnetic field-aligned, strahl electrons have pitch angle distributions which become broader in width as electron kinetic energy increases. Magnetosonic-whistler waves propagating sunward at k × B o = 0 where B o is the background magnetic field and k is the wave number have a cyclotron resonance with electrons propagating in the anti-sunward direction. This resonance leads to pitch angle scattering which increases strahl electron energy perpendicular to B o . The strahl response to a broadband whistler fluctuation spectrum was studied using Particle-In-Cell (PIC) simulations in a magnetized, homogeneous, collisionless plasma. The simulations show that enhanced whistler waves with finite damping lead to strahl pitch angle distributions which broaden in width with increasing kinetic energy, in agreement with certain observations. Results from the simulations show how the strahl is broadened as a function of wave amplitude and relative strahl density.

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